Context : NGC 2682 is a nearby open cluster , approximately 3.5 Gyr old .
Dynamically , most open clusters should dissolve on shorter timescales , of \approx 1 Gyr .
Having survived until now , NGC 2682 was likely much more massive in the past , and is bound to have an interesting dynamical history .

Aims : We investigate the spatial distribution of NGC 2682 stars to constrain its dynamical evolution , especially focusing on the marginally bound stars in the cluster outskirts .

Methods : We use Gaia DR2 data to identify NGC 2682 members up to a distance of \sim 150 pc ( 10 degrees ) .
Two methods ( Clusterix and UPMASK ) are applied to this end .
We estimate distances to obtain three-dimensional stellar positions using a Bayesian approach to parallax inversion , with an appropriate prior for star clusters .
We calculate the orbit of NGC 2682 using the GRAVPOT16 software .

Results : The cluster extends up to 200′ ( 50 pc ) which implies that its size is at least twice as previously believed .
This exceeds the cluster Hill sphere based on the Galactic potential at the distance of NGC 2682 .

Conclusions : The extra-tidal stars in NGC 2682 may originate from external perturbations such as disk shocking or dynamical evaporation from two-body relaxation .
The former origin is plausible given the orbit of NGC 2682 , which crossed the Galactic disk \approx 40 Myr ago .