  The formation and evolution of an X--ray cluster is studied using a 3--D
N-body + hydrodynamical simulation which includes feedback of energy and iron
from cluster galaxies. The differences in evolution and final state between the
simulation and a similar run without feedback are highlighted. We address the
energetics of cluster gas; the distribution of dark matter, gas, and galaxies;
the thermodynamic state of cluster gas, the beta model, and the beta
discrepancy; x-ray evolution; the validity of estimates of the binding mass and
of the baryon fraction of the cluster; dynamics of the galaxy population and
velocity bias; and of the evolution of the iron abundance distribution in the
cluster. We find that preheating by galactic winds results in a lower core
density for the ICM, which in turn makes the simulated cluster fainter at high
redshift and undergo rapid luminosity evolution to the present. A strong iron
abundance gradient is present, even at high redshift. Velocity bias is present
in the galaxy population; this bias combined with the preheating from winds
drives the value of $\beta_{spec}\,=\,\sigma^{2}/\left(kT/\mu m_{p}\right)$ to
values less than one. The two fluid simulation, modelling infall only, predicts
$\beta_{spec}\,\geq\,1$, less in line with observation.
