  The collective properties of star clusters are investigated using a
simulation of the collision between two dwarf galaxies. The characteristic
power law of the cluster mass function, N(M), with a slope dlog N/dlog M ~ -1,
is present from cluster birth and remains throughout the simulation. The
maximum mass of a young cluster scales with the star formation rate (SFR). The
relative average minimum separation, R(M)= N(M)^{1/p}D_min(M)/D(M_low), for
average minimum distance D_min(M) between clusters of mass M, and for lowest
mass, M_low, measured in projection (p=2) or three dimensions (p=3), has a
negative slope, dlog R/dlog M ~ -0.2, for all masses and ages. This agrees with
observations of R(M) in low-mass galaxies studied previously. Like the slope of
N(M), R}(M) is apparently a property of cluster birth for dwarf galaxies that
does not depend on SFR or time. The negative slope for R(M) implies that more
massive clusters are centrally concentrated relative to lower mass clusters
throughout the entire mass range. Cluster growth through coalescence is also
investigated. The ratio of the kinetic to potential energy of all near-neighbor
clusters is generally large, but a tail of low values in the distribution of
this ratio suggests that a fraction of the clusters merge, ~8% by number
throughout the ~300 Myr of the simulation and up to 60% by mass for young
clusters in their first 10 Myr, scaling with the SFR above a certain threshold.
