  The processes that lead from molecular clouds to protostars, stellar
associations, and the evolution of both, are active research topics. The target
of this study, NGC2264, is a benchmark star-forming region (SFR) in which these
issues can be profitably studied.
  We assembled a new extensive sample of NGC 2264 members. To this end we used
new X-ray data obtained with the XMM-Newton telescope, GAIA eDR3 data, and an
extensive collection of public and published catalogs. Following a previous
suggestion that the SFR might extend significantly beyond the better studied
areas, our search covers a wide 2.5x2.5 degrees region in the sky.
  Our catalog comprises more than 2200 candidate members, a ~100% increase over
previous determinations. We analyze their spatial distribution and define new
substructures. Using GAIA parallaxes we estimate a new average distance to
NGC2264 of 722+/-2pc and suggest that the embedded Spokes subregion is ~20pc
farther away within the molecular cloud. A complex dynamics is unveiled by the
available proper motions and radial velocities: we observe signs of global
expansion and rotation. At the same time, we observe the collapse and
coalescence of two substructures in a region where active star formation is
taking place. The fraction of stars with disks and of those undergoing
circumstellar accretion varies significantly across the field, suggesting that
star formation has been occurring for several million years. A particularly low
disk fraction around the O VII star S Mon might be attributed to external disk
photoevaporation or to an older age of the stars in the region.
  NGC2264 is not dynamically relaxed and its present configuration is the
result of multiple dynamical processes. The cloud has been forming stars for
several million years and we identify the process that is likely responsible
for the ongoing formation activity.
