We present a multi-wavelength analysis of the galaxies in nine clusters selected from the WINGS dataset, examining how galaxy structure varies as a function of wavelength and environment using the state of the art software GALAPAGOS-2 . We simultaneously fit single-Sérsic functions on three optical ( u , B and V ) and two near-infrared ( J and K ) bands thus creating a wavelength-dependent model of each galaxy. We measure the magnitudes, effective radius ( R e ), the Sérsic index ( n ), axis ratio, and position angle in each band. The sample contains 790 cluster members (located close to the cluster centre < 0.64 ×  R 200 ) and 254 non-member galaxies that we further separate based on their morphology into ellipticals, lenticulars, and spirals. We find that the Sérsic index of all galaxies inside clusters remains nearly constant with wavelength while R e decreases as wavelength increases for all morphological types. We do not observe a significant variation on n and R e as a function of projected local density and distance from the clusters centre. Comparing the n and R e of bright cluster galaxies with a subsample of non-member galaxies we find that bright cluster galaxies are more concentrated (display high n values) and are more compact (low R e ). Moreover, the light profile ( ) and size (ℛ) of bright cluster galaxies does not change as a function of wavelength in the same manner as non-member galaxies.