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Exploring the Galactic chemical evolution and enrichment scenarios with openclusters allows us to understand the history of the Milky Way disk.High-resolution spectra of OCs are a crucial tool, as they provide precisechemical information, to combine with precise distances and ages. The aim ofthe Stellar Population Astrophysics project is to derive homogeneous andaccurate comprehensive chemical characterization of a number of poorly studiedOCs.Using the HARPS-N echelle spectrograph at the Telescopio Nazionale Galileo,we obtained high-resolution spectra of giant stars in 18 OCs, 16 of which arechemically characterized for the first time, and two of which are well studiedfor comparison. The OCs in this sample have ages from a few tens of Myr to 4Gyr, with a prevalence of young clusters. We already presented the radialvelocities and atmospheric parameters for them in a previous SPA paper. Here,we present results for the alpha-elements O, and the light elements, alldetermined by the equivalent width method. We also measured Li abundancethrough the synthesis method.We discuss the behaviors of lithium, sodium andaluminum in the context of stellar evolution. We study the radial, vertical,and age trends for the measured abundance ratios in a sample that combines ourresults and recent literature for OCs, finding significant gradients only for[Mg/Fe] and [Ca/Fe] in all cases. Finally,we compare O and Mg in the combinedsample with chemo-dynamical models, finding a good agreement forintermediate-age and old clusters. There is a sharp increase in the abundanceratios measured among very young clusters, accompanied by a poorer fit with themodels for O and Mg, likely related to the inadequacy of traditional modelatmospheres and methods in the derivation of atmospheric parameters andabundance ratios for stars of such young ages

Stellar Population Astrophysics (SPA) with the TNG. alpha-elements, lithium, sodium and aluminum in 16 open clusters