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In a previous paper we introduced a new method for simulating collisionalgravitational $N$-body systems with linear time scaling on $N$, based on theMulti-Particle Collision (MPC) approach. This allows us to simulate globularclusters with a realistic number of stellar particles in a matter of hours on atypical workstation. We evolve star clusters containing up to $10^6$ stars tocore collapse and beyond. We quantify several aspects of core collapse overmultiple realizations and different parameters, while always resolving thecluster core with a realistic number of particles. We run a large set of N-bodysimulations with our new code. The cluster mass function is a power-law with nostellar evolution, allowing us to clearly measure the effects of the massspectrum. Leading up to core collapse, we find a power-law relation between thesize of the core and the time left to core collapse. Our simulations thusconfirm the theoretical self-similar contraction picture but with a dependenceon the slope of the mass function. The time of core collapse has anon-monotonic dependence on the slope, which is well fit by a parabola. Thisholds also for the depth of core collapse and for the dynamical frictiontimescale of heavy particles. Cluster density profiles at core collapse show abroken power law structure, suggesting that central cusps are a genuine featureof collapsed cores. The core bounces back after collapse, and the inner densityslope evolves to an asymptotic value. The presence of an intermediate-massblack hole inhibits core collapse. We confirm and expand on several predictionsof star cluster evolution before, during, and after core collapse. Suchpredictions were based on theoretical calculations or small-size direct$N$-body simulations. Here we put them to the test on MPC simulations with amuch larger number of particles, allowing us to resolve the collapsing core.

Introducing a new multi-particle collision method for the evolution of dense stellar systems II. Core collapse