  We use two high resolution CDM simulations to show that (i) when clusters of
galaxies form the infall pattern of matter is not random but shows clear
features which are correlated in time; (ii) in addition, the infall patterns
are correlated with the cluster's surrounding Large Scale Structure; (iii)
Large Scale Structure shows a mix of both filaments and sheets; (iv) the amount
of mass in filaments is slightly larger for a low $\Omega$ model.
