We report astrophysical properties of 12 Milky Way open clusters located beyond a 2 kpc circle around the Sun by using deep optical photometry .
We estimated their age and metallicities on the basis of a maximum likelihood approach using astrometric members determined from Gaia DR2 data .
The studied clusters turned out to be of intermediate-age ( 0.8 - 4.0 Gyr ) , with metallicities spanning the range [ Fe/H ] \sim -0.5 - +0.1 dex , and distributed within the general observed trend of the Milky Way disc radial and perpendicular metallicity gradients .
As far as we are aware , these are the first metal abundance estimates derived for these clusters so far .
From the constructed stellar density radial profiles and cluster mass functions we obtained a variety of structural and internal dynamics evolution parameters .
They show that while the innermost cluster regions would seem to be mainly shaped according to the respective internal dynamics evolutionary stages , the outermost ones would seem to be slightly more sensitive to the Milky Way tidal field .
The nearly coeval studied clusters are experiencing different levels of two-body relaxation following star evaporation ; those at more advanced stages being more compact objects .
Likewise , we found that the more important the Milky way tides , the larger the Jacobi volume occupied by the clusters , irrespective of their actual sizes and internal dynamics evolutionary stages .