  Thanks to the rapid progress in precision cosmology in the last few years, we
now have access to physical observables that may constrain the theory of
inflation through the non-Gaussianity (NG) signatures in the cosmic microwave
background radiation and the distribution of large-scale structure. Numerical
modeling of the NG signals from different inflation models is essential to
correctly interpret current and near future data from large-scale structure
surveys. In this study, we use high-resolution cosmological hydrodynamical
simulations to investigate the effects of primordial NG on the formation and
evolution of galaxies from the cosmic dawn to the present day. Focusing on the
local type primordial NG, we find that it may affect the formation history of
stars and black holes in galaxies, and their distribution. Compared to the
Gaussian case, large non-Gaussian potential with $f_{NL} \gtrsim 10^3$ leads to
earlier collapse of the first structures, more massive galaxies especially at
high redshifts, stronger clustering of galaxies, and higher halo bias. However,
for smaller NG with $f_{NL} \lesssim 10^2$, the effect is significantly weaker.
Observations of the distribution and properties of high-redshift, rare objects
such as the first galaxies and quasars may provide further constraints on the
primordial NG.
