  This work is focused on the study of the distribution in the CPPS of passive
and star-forming galaxy populations and also, the intense and quiescent
star-forming populations for a set of 9 nearby z<0.05 galaxy clusters.
Furthermore, we compare the CPPS distribution of the passive galaxy population
with the accreted halo population of a set of 28 simulated clusters and the
star-forming population with the non-accreted population. We consider various
cluster accretion epochs and accretion radii where it is assumed that star
formation in galaxies becomes quenched, in order to segregate the accreted
population from the non-accreted population. Just applying this segregation in
simulations, we get a qualitative agreement between the CPPS distributions of
the passive and the accreted populations and also between the star-forming and
the non-accreted populations. The uncertainty in cluster centering strongly
affects the pronounced cuspy profiles of the projected density and also, it can
explain the main difference (i.e. inner slope) between the CPPS distribution of
passive and accreted populations. The CPPS density of star-forming galaxies and
the intensity of ram-pressure stripping present an opposite trend throughout
the CPPS. This implies that ram-pressure stripping significantly contributes to
modulate the observed CPPS distribution of star-forming galaxies inside and
around cluster virial regions. The significant fraction of star-forming
galaxies at the projected center of clusters are mainly those galaxies with low
l-o-s velocities and they can be mainly identified as those galaxies with a
remaining star formation activity (quiescent star-forming galaxies) inside the
physical virial region or, in a lower degree, as galaxy interlopers i.e.
outside the physical virial region.(abridged)
