  We explore galaxy properties and their link with environment and clustering
using a population of ~1000 galaxies formed in a high resolution hydrodynamic
simulation of the Lambda CDM cosmology. At the redshift we concentrate on, z=1,
the spatial resolution is 1.4 proper kpc/h and Milky-way sized disk galaxies
contain ~10^5 particles within their virial radii. We include supermassive
black hole accretion and feedback as well as a multiphase model for star
formation. We find that a number of familiar qualitative relationships hold
approximately between galaxy properties, for example, galaxies lie between two
broad extremes of type, where ``late'' types tend to be smaller in size, have
lower circular velocities, younger stars, higher star formation rates, larger
disk to bulge ratios and lower Sersic indices than ``early types''. As in
previous studies the stellar component of disk galaxies is not as rotationally
supported as in observations. Bulges contain too much of the stellar mass,
although disks do have scale lengths compatible with observations. The addition
of black hole physics to the simulations does not appear to have an impact on
the angular momentum results, nor do we find that it is affected in an
identical simulation with significantly lower mass resolution. Despite this, we
can profitably use the rank order of either disk to total ratio, Sersic index,
or galaxy age to separate galaxies into morphological classes and examine the
density-morphology relation and morphology dependence of clustering. We find
that while at redshift z=0, the well known preponderance of early types in
dense environments is seen, at z=1 the density-morphology relation becomes
flatter and late type galaxies are even seen to have a higher clustering
amplitude than early types (abridged).
