  We model the collision of molecular clouds to investigate the role of the
initial properties on the remnants. Our clouds collide and evolve in a
background medium that is approximately ten times less dense than the clouds,
and we show that this relatively dense background is dynamically important for
the evolution of the collision remnants. Given the motion of the clouds and the
remnants through the background, we develop, implement, and introduce dynamic
boundary conditions. We investigate the effect of the initial cloud mass,
velocity, internal turbulence, and impact angle. The initial velocity and its
velocity components have the largest affect on the remnant. This affects the
spatial extent of the remnant, which affects the number of resulting star
clusters and the distribution of their masses. The less extended remnants tend
to have fewer, but more massive, clusters. Unlike the clusters, the gas
distributions are relatively insensitive to the initial conditions, both the
distribution of the bulk gas properties and the gas clumps. In general, cloud
collisions are relatively insensitive to their initial conditions when modelled
hydrodynamically in a dynamically important background medium.
