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[Abridged] We investigate the frequency of the various spectral types as afunction both of the clusters' properties and of the galaxies' characteristics.In this way, using the same classification criteria adopted for higher redshiftstudies, we can consistently compare the properties of the local clusterpopulation to those of their more distant counterparts. We describe a method wehave developed to automatically measure the equivalent width of spectral linesin a robust way even in spectra with a non optimal signal to noise. Like this,we can derive a spectral classification reflecting the stellar content, basedon the presence and strength of the [OII] and Hdelta lines. We are able tomeasure 4381 of the ~6000 originally observed spectra, in the fields of 48clusters, 2744 of which are spectroscopically confirmed cluster members. Thespectral classification is then analyzed as a function of galaxies' luminosity,stellar mass, morphology, local density and host cluster's global properties,and compared to higher redshift samples (MORPHS and EDisCS). The vast majorityof galaxies in the local clusters population are passive objects, being alsothe most luminous and massive. At a magnitude limit of Mv<-18, galaxies in apost-starburst phase represent only ~11% of the cluster population and thisfraction is reduced to ~5% at Mv<-19.5, which compares to the 18% at the samemagnitude limit for high-z clusters. "Normal" star forming galaxies [e( c )]are proportionally more common in local clusters. The relative occurrence ofpost--starbursts suggests a very similar quenching efficiency in clusters atredshifts in the 0 to ~1 range. Furthermore, more important than the globalenvironment, the local density seems to be the main driver of galaxy evolutionin local clusters, at least with respect to their stellar populations content.

WINGS-SPE III: Equivalent width measurements, spectral properties and evolution of local cluster galaxies