  We present a new, deep (V ~ 26) study of the Galactic globular cluster NGC
2419 based on B,V,I time-series CCD photometry over about 10 years and
extending beyond the cluster published tidal radius. We have identified 101
variable stars of which 60 are new discoveries, doubling the known RR Lyrae
stars and including 12 SX Phoenicis stars. The average period of the RR Lyrae
stars (<Pab>=0.662 d, and <Pc>=0.366 d, for fundamental-mode -RRab- and
first-overtone pulsators, respectively), and the position in the
period-amplitude diagram both confirm that NGC 2419 is an Oosterhoff II
cluster. The average apparent magnitude of the RR Lyrae stars is <V>=20.31 +/-
0.01 (sigma=0.06, 67 stars) and leads to the distance modulus (m-M)o=19.60 +/-
0.05. The Color-Magnitude Diagram, reaching about 2.6 mag below the cluster
turn-off, does not show clear evidence of multiple stellar populations. Cluster
stars are found until r~ 10.5', and possibly as far as r~15', suggesting that
the literature tidal radius might be underestimated. No extra-tidal structures
are clearly detected in the data. NGC 2419 has many blue stragglers and a well
populated horizontal branch extending from the RR Lyrae stars down to an
extremely blue tail ending with the "blue-hook", for the first time recognized
in this cluster. The red giant branch is narrow ruling out significant
metallicity spreads. Our results seem to disfavor the interpretation of NGC
2419 as either having an extragalactic origin or being the relict of a dwarf
galaxy tidally disrupted by the Milky Way.
