The distribution of the stars in a stellar cluster is the consequence of the dynamical evolution along its lifetime affected by internal and external mechanisms. Particularly, open clusters allow to investigate the dynamical evolution of systems with a small number of objects. The fact that a cluster survives or dissolves depends on its initial mass but also of the interactions with external structures such as the disk. Dynamical models predict that a cluster with the typical mass of a bound open cluster would be dissolved in a timescale lower than 1 Gyr. Although a minority, there are a significant number of open cluster older than 1 Gyr. They are key to investigate the dynamical evolution of clusters, and the balance among self gravity, internal dynamics, and external tidal forces. In this talk I will present the results of our study of the 3.5 Gyr old open cluster NGC 2682 (M67) structure taken advantage the high quality astrometric information provided by the second data release of the Gaia mission.