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The Six Day's Ephemeris summarizes A Brief History of Time as follows:
Working backwards from the present state of the Universe, scientists hypothesize that it must have begun as a single point of infinite density and finite time that began to expand. According to the theory, after the initial expansion, the Universe cooled sufficiently to allow the formation of subatomic particles, and later simple atoms. Giant clouds of these primordial elements later gravitationally coalesced to form stars and galaxies.
This all started around 13.8 billion years ago, and is thus considered the Universe's age. Scientists have constructed a timeline of events that began with the Big Bang and has led to the current state of cosmic evolution by testing theoretical principles, experiments involving particle accelerators and high-energy states, and astronomical studies that have observed the deep Universe.
The earliest times of the Universe, however, ranging from approximately 10^ (-43) to 10^ (-11) seconds after the Big Bang, are the subject of much speculation. Given that the known laws of physics could not exist at this time, it is difficult to imagine how the Universe could have been governed. Furthermore, no experiments that can generate the types of energies involved have been conducted. Even so, many theories about what happened in that first instant of time exist, with many of them being compatible. The Six Day Ephemeris can be summed up as follows:

The Day of Dawn:
The Big Bang Day.
In the beginning, there was a single primeval atom outside the frame of space and time, which consisted of all the matter and energy of our current Universe. Also known as the Planck Epoch (or Planck Era); this was the earliest known period of the Universe. During this Era, it is believed that the quantum effects of gravity dominated physical interactions.
This Planck period of time extends from point 0 to approximately 10 ^ (-43) seconds, and is so named because it can only be measured in Planck time . Due to the extreme heat and density of matter, the state of the Universe was highly unstable. It thus began to expand and cool, leading to the manifestation of the fundamental forces of physics.
For reasons that we do not know, and perhaps will never know, this Primeval Atom went through a superfast inflation. From approximately 10^ (-43) second to 10^ (-36) second, the Universe began to cross transition temperatures. It is here that the fundamental forces that govern the Universe are believed to have begun separating from each other. The first step in this was the force of gravitation separating from gauge forces, which account for strong and weak nuclear forces and electromagnetism. Then, from 10^ (-36) to 10^ (-11) seconds after the Big Bang, the temperature of the Universe was low enough (1028 K) that the forces of electromagnetism (strong force) and weak nuclear forces (weak interaction) were able to separate as well, forming two distinct forces.
Thus, the clock of time began to tickle. If we had a time machine today that allowed us to go back in time about 13.8 billion years, we would return to the point from which the Universe began. No one knows what happened in or before the first second of the Universe's birth, as our known cosmic laws do not apply to that era.

As the density and temperature of the Universe decreased, so did the energy of each particle, and phase transitions continued until the fundamental forces of physics and elementary particles changed into their current form. This period is less speculative because particle energies would have dropped to values that particle physics experiments can obtain.
Scientists believe that about 10^ (-11) seconds after the Big Bang, particle energies dropped considerably. At about 10^ (-6) seconds, quarks and gluons combined to form baryons such as protons and neutrons, and a small excess of quarks over antiquarks led to a small excess of baryons over antibaryons.
Since temperatures were not high enough to create new proton-antiproton pairs (or neutron-antineutron pairs), mass annihilation immediately followed, leaving just one in 1010 of the original protons and neutrons and none of their antiparticles. A similar process happened at about 1 second after the Big Bang for electrons and positrons. After these annihilations, the remaining protons, neutrons and electrons were no longer moving relativistically and the energy density of the Universe was dominated by photons – and to a lesser extent, neutrinos. In this stage nucleosynthesis also began, it has taken place in the interval from roughly 10 seconds to 20 minutes after the Big Bang, and is calculated to be responsible for the formation of most of the Universe's helium as the isotope helium-4 (4He), along with small amounts of the hydrogen isotope deuterium (2H or D).
Thanks to temperatures dropping to 1 billion kelvins and the energy densities dropping considerably, neutrons and protons began to combine to form the Universe's first deuterium (a stable isotope of Hydrogen) and helium atoms. However, most of the Universe's protons remained uncombined as hydrogen nuclei.

The Second Day:
Let it be light.
This day begins 379,000 years after the birth of the Universe. Electrons combined with their nuclei to form atoms (again, mostly hydrogen), while the radiation decoupled from matter and continued to expand through space, largely unimpeded. This radiation is now known to be what constitutes the Cosmic Microwave Background (CMB), which today is the oldest light in the Universe.
As the CMB expanded, it gradually lost density and energy, and is currently estimated to have a temperature of 2.7260 ± 0.0013 K (-270.424 °C/ -454.763 °F) and an energy density of 0.25 eV/cm3 (or 4.005×10-14 J/m3; 400–500 photons/cm3). The CMB can be seen in all directions at a distance of roughly 13.8 billion light years, but estimates of its actual distance are at about 46 billion light years from the center of the Universe. This background radiation is the most important trace that remains from the first and second days of creation.
Inflation continued at its superfast speed, the inflation fragments continued to diverge thus continuing to weave space and time, the Universe at that time had cooled to about 3000 degrees Kelvin (about 2700 degrees Celsius), which allowed the electrons to be attracted to their protons allowing them to appear for the first time in a state of extreme agitation that led to the emission of a torrent of photons, allowing the first visible rays of light to appear.

The map of the Universe above shows the Universe's first emergence, or cosmic radiation background, printed on the sky when the Universe was 379,000 years old. The chart shows tiny temperature fluctuations across the sky, corresponding to a hue from white to black. The dark regions are cooler compared to the light regions. This map will bear the seeds of the structure of the world in the following years and how stars and galaxies are distributed.