  We discuss evidence in local, present-day clusters of galaxies (from the
ENACS survey) about the way in which those clusters have evolved and about the
evolutionary relationships between the galaxies of different morphological
types in them. This evidence is complementary to that obtained from the study
of clusters at intermediate and high redshifts. We argue that the spatial
distribution and the kinematics of the various types of galaxies in and outside
substructures support the following picture.
  The ELLIPTICAL AND S0 GALAXIES have been around for a long time and have
obtained an isotropic velocity distribution. The spatial distribution and
kinematics of the EARLY SPIRALS are consistent with the idea that many of their
kind have transformed into an S0, but that they have survived, most likely
because of their velocities. The distribution and kinematics of the LATE
SPIRALS are consistent with a picture in which they have been accreted fairly
recently. They have mildly radial orbits and hardly populate the central
regions, most likely because they suffer tidal disruption. Finally, the
distribution and kinematics of the GALAXIES IN SUBSTRUCTURES, when taken at
face value, imply tangential velocity anisotropy for these galaxies, but this
result may be (partly) due to the procedure by which these galaxies are
selected. A first attempt to take the effects of selection into account shows
that isotropic (or even mildly radial) orbits of subcluster galaxies cannot be
excluded.
