  The formation history of rich clusters is investigated using a hybrid N-body
simulation in which high spatial and mass resolution can be achieved
self-consistently within a small region of a very large volume. The evolution
of three massive clusters is studied via mass accretion, spherically-averaged
density profiles, three-dimensional and projected shapes, and degree of
substructure. Each cluster consists of order $4\times 10^5$ particles at the
present epoch and in the case that rich cluster evolution is well-described by
a 1-parameter family, the simulations have sufficient resolution to demonstrate
this. At $z=0$ the clusters have similar masses, $M(r \le 1.5h^{-1} Mpc) \sim
2\times 10^{15} h^{-1} M_\odot$, and similar spherically-averaged density
profiles, however markedly different formation histories are observed. No
single, dominant pattern is apparent in the time variation of the mass
accretion rate, the cluster shape, or the degree of substructure. Although not
a statistically large sample, these objects suggest that the detailed formation
history of rich clusters cannot be characterized by a simple 1-parameter
family. These results suggest that the use of observations of rich clusters
over a wide range of redshifts to constrain cosmological parameters may not be
entirely straightforward.
