  (Abridged) The lifetime of protoplanetary disks around young stars limits the
timescale when planets form. A disk dissipation timescale < 10 Myr was inferred
from surveys providing the fraction of stars with disks in young stellar
clusters with different ages. However, most previous surveys focused on the
compact region within ~ 2 pc from the clusters' centers, for which the disk
fraction information considering the outer part is practically absent. We aim
to test if disk fraction estimates change when inferred from an extended region
around the clusters' centers. Gaia EDR3 data and a best-suited, Virtual
Observatory (VO)-based tool -Clusterix-, are used to identify member stars for
a representative sample of 19 young clusters considering two concentric fields
of view (FOV) with radii ~ 20 pc and ~ 2 pc. Our analysis reveals that the
inner disk fractions inferred from the compact and the extended regions are
equal within ~ 10%, which does not support a previous hypothesis proposing that
disk fractions should be significantly larger considering extended regions. A
list of member and disk stars in each cluster is provided and stored in a
VO-compliant archive. Averaged values and plots characterizing the whole
clusters are also provided, including HR diagrams based on Gaia colors and
absolute magnitudes. Our results cover the largest fields ever probed when
dealing with disk fractions for all clusters analysed, and imply that their
complete characterization requires the use of wide FOVs. The resulting database
is a benchmark for future detailed studies of young clusters, whose disk
fractions must be accurately determined by using multi-wavelength analysis
potentially combined with data from coming Gaia releases.
