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In this third paper in our cloud-collision series, we present the resultsfrom simulations of head-on collisions with a strongly centrally-condensedinitial density profile of $\rm \rho \propto R^{-2}$. We investigate the impactof these density profiles on the overall evolution of the simulations: thestructures formed, their dynamical evolution, and their star formationactivity. We consider clouds which are globally bound and globally unbound,leading to three different scenarios -- the collision of a bound cloud with abound cloud, the collision of two unbound clouds, or the collision of one cloudof each type. In all the simulations dense star clusters form before thecollisions occur, and we find that star formation remains confined to thesesystems and is little affected by the collisions. If the clouds' are bothinitially bound, the collision forms a filamentary structure, but otherwise,this does not occur. We observe that rotating structures form around theclusters, but they also form in our non-colliding control simulations, so arenot a consequence of the collisions. Dissipation of kinetic energy in thesesimulations is inefficient because of the substructure created in the clouds byturbulence before the collisions. As a result, although some gas is left boundin the COM frame, the star clusters formed in the simulations do not becomebound to each other.

Collision Between Molecular Clouds-III: The effects of cloud initial density profile on head-on collisions