  NASA's TESS mission is expected to discover hundreds of M dwarf planets.
However, few studies focus on how planets form around low-mass stars. We aim to
better characterize the formation process of M dwarf planets to fill this gap
and aid in the interpretation of TESS results. We use ten sets of N-body planet
formation simulations which vary in whether a gas disc is present, initial
range of embryo semi-major axes, and initial solid surface density profile.
Each simulation begins with 147 equal-mass embryos around a 0.2 solar mass star
and runs for 100 Myr. We find that planets form rapidly, with most collisions
occurring within the first 1 Myr. The presence of a gas disc reduces the final
number of planets relative to a gas-free environment and causes planets to
migrate inward. We find that roughly a quarter of planetary systems experience
their final giant impact inside the gas disc, suggesting that some super-Earths
may be able to reaccrete an extended gaseous envelope after their final giant
impact, though these may be affected by additional process such as
photoevaporation. In addition, we find that the final distribution of planets
does not retain a memory of the slope of the initial surface density profile,
regardless of whether or not a gas disc is present. Thus, our results suggest
that present-day observations are unlikely to provide sufficient information to
accurately reverse-engineer the initial distribution of solids.
