Planets form in “protoplanetary” disks around young stars. Thus, establishing an accurate disk dissipation timescale is key to constraint the maximum period available for planet formation. That timescale is smaller than ~ 10 Myr, based on surveys counting the relative number of stars with disks -the disk fraction- in young clusters with different ages. Gaia is revolutionising the study of clusters thanks to its accurate proper motion and parallax measurements. In particular, Gaia’s data have supported that most clusters expand during the critical period when disks dissipate. It was hypothesized that due to this expansion and the relatively narrow fields of view (FOVs) used in most surveys measuring the disk fraction, the inferred disk dissipation timescale could be significantly underestimated because only the disks in the densest regions of the clusters were considered. We are testing this hypothesis by comparing the disk fractions estimated from two FOVs with radii corresponding to ~ 2 and ~ 20 pc from the centers of a representative sample of young clusters. Gaia EDR3 parallaxes and proper motions, along with a best suited tool (Clusterix: http://clusterix.cab.inta-csic.es/clusterix/), are being used for membership determination. JHK color-color diagrams serve to compare the disk fractions derived considering both spatial scales around the young stellar clusters. This poster presents the results of our ongoing work.