  We use high resolution PM N-body simulations to follow the development of
non-linear clustering in a flat Universe, dominated by Cold + Hot Dark Matter
(CHDM) with 60% of CDM, 30% of HDM and 10% of baryons; a simulation box of 100
Mpc a side ($h=0.5$) is used. We analyze two CHDM simulations with $b =1.5$
(COBE normalization). We also compare them with CDM simulations with $b=1.5$
and $b=1$. We evaluate high-order correlation functions and the
void-probability-function (VPF). Correlation functions are obtained both from
counts in cells and counts of neighbors. The analysis is made for DM particles
and for galaxies, identified as massive halos in the evolved density field. We
also check the effects of dynamical evolution and redshift space distortions.
We find that clustering of DM particles exhibits deviations from the
hierarchical scaling, which decrease somewhat in redshift space. Galaxies
follow hierarchical scaling far more closely, with coefficients S_3=2.5 and
S_4=7.5, in general agreement with observational results, just marginally
affected by redshift distortions and on the choices for the initial spectra.
The hierarchical scaling of galaxy clustering is confirmed by the VPF analysis
and in all the cases considered a good agreement with observational results is
obtained.
