  We study the structure and the internal colour gradients of cluster galaxies
from UV to NIR restframe, in the redshift range z=0.21-0.64. Structural
parameters (half light radius r_e, mean surface brightness mu_e and Sersic
index n) are derived. This data set constitutes the first large (N ~ 270)
sample of cluster galaxies whose internal structure in UV, optical (OPT) and
NIR (U-, V- and H-band restframe) can be investigated up to a look-back time of
~6 Gyr (Omega_m=0.3, Omega_Lambda=0.7 and H_0=70 Km/s/Mpc). Galaxies are
classified as spheroids or disks according to the shape of the light profile,
and the evolution of the two populations are investigated separately. On
average, both spheroids and disks are more concentrated at longer wavelengths:
the galaxy sizes become smaller from UV to NIR, while Sersic indices increase.
This trend shows an evolution in disks, where the mean ratio of optical to NIR
Sersic indices decreases from z=0.31 to z=0.64. Colour gradients are on average
negative at all redshifts and are stronger in disks than in spheroids.
  Colour gradients and central colours are compared with models of metallicity,
age, and dust extinction gradients. Metallicity turns out to be the primary
driver of colour gradients in spheroids, the age gradient being constrained to
be smaller than ~25%. For disks, two kinds of models fit the present data: (i)
age gradients (in the range [30,50]%) with significant dust extinction, and
(ii) `pure' dust models, in which the gradients of colour excess are a factor
of two higher in EIS 0048 than in the other clusters. Since colour gradients of
disks seem not to correlate significantly with inclination, we argue that age
gradient models could represent a more likely explanation of the present data,
in agreement with what expected on the basis of hierarchical merging scenarios.
