  We analyze a new large-scale ($100h^{-1}$Mpc) numerical hydrodynamic
simulation of the popular $\Lambda$CDM cosmological model, including in our
treatment dark matter, gas and star-formation, on the basis of standard
physical processes. The method, applied with a numerical resolution of
$<200h^{-1}$kpc (which is still quite coarse for following individual galaxies,
especially in dense regions), attempts to estimate where and when galaxies
form. We then compare the smoothed galaxy distribution with the smoothed mass
distribution to determine the "bias" defined as $b\equiv (\delta
M/M)_{gal}/(\delta M/M)_{total}$ on scales large compared with the code
numerical resolution (on the basis of resolution tests given in the appendix of
this paper). We find that (holding all variables constant except the quoted
one) bias increases with decreasing scale, with increasing galactic age or
metallicity and with increasing redshift of observations. At the $8h^{-1}$Mpc
fiducial comoving scale bias (for bright regions) is 1.35 at $z=0$ reaching to
3.6 at $z=3$, both numbers being consistent with extant observations. We also
find that $(10-20)h^{-1}$Mpc voids in the distribution of luminous objects are
as observed (i.e., observed voids are not an argument against CDM-like models)
and finally that the younger systems should show a colder Hubble flow than do
the early type galaxies (a testable proposition). Surprisingly, little
evolution is found in the amplitude of the smoothed galaxy-galaxy correlation
function (as a function of {\it comoving} separation). Testing this prediction
vs observations will allow a comparison between this work and that of Kauffmann
et al which is based on a different physical modelingmethod.
