We present UBVRI photometry of the open cluster NGC2422 (age∼ 108 yr) down to a limiting magnitude V 19. These data are used to derive the Luminosity and Mass Functions and to study the cluster spatial distribution. By considering the color–magnitude diagram data and adopting a representative cluster main sequence, we obtained a list of candidate cluster members based on a photometric criterion. Using a reference field region and an iterative procedure, a correction for contaminating field stars has been derived in order to obtain the Luminosity and the Mass Functions in the M = 0.4−3.5 M range. By fitting the spatial distribution, we infer that a non-negligible number of cluster stars lies outside our investigated region. We have estimated a correction to the Mass Function of the cluster in order to take into account the “missing” cluster stars. The Present Day Mass Function of NGC2422 can be represented by a power-law of index α = 3.07 ± 0.08 (rms) – the Salpeter Mass Function in this notation has index α = 2.35 – in the mass range 0.9 ≤ M/M ≤ 2.5. The index α and the total mass of the cluster are very similar to those of the Pleiades.