  We have identified over 2000 well resolved cluster halos, and also their
associated bound subhalos, from the output of a 1024^3 particle cosmological
N-body simulation (of box size 320 h^-1 Mpc and softening length 3.2 h^-1 kpc).
This has allowed us to measure halo quantities in a statistically meaningful
way, and for the first time analyse their distribution for a large and well
resolved sample. We characterize each halo in terms of its morphology,
concentration, spin, circular velocity and the fraction of their mass in
substructure. We also identify those halos that have not yet reached a state of
dynamical equilibrium using the virial theorem with an additional correction to
account for the surface pressure at the boundary. These amount to 3.4% of our
initial sample. For the virialized halos, we find a median of 5.6% of halo mass
is contained within substructure, with the distribution ranging between no
identified subhalos to 65%. The fraction of mass in substructure increases with
halo mass with logarithmic slope of 0.44 +- 0.06. Halos tend to have a prolate
morphology, becoming more so with increasing mass. Subhalos have a greater
orbital angular momentum per unit mass than their host halo. Furthermore, their
orbital angular momentum is typically well aligned with that of their host.
Overall, we find that dimensionless properties of dark matter halos do depend
on their mass, thereby demonstrating a lack of self-similarity.
