  Using UBVRI Halpha CCD photometric observations and the archival NIR and
X-ray data, we have carried out a multi-wavelength study of a young star
cluster NGC 7419. An age of 22.5+/-3.0 Myr and a distance of 3230^{+330}_{-430}
pc are derived for the cluster with a higher value of color excess ratio
E(U-B)/E(B-V) than the normal one. There is an evidence for mass segregation in
this dynamically relaxed cluster with mass function slope is in agreement with
the Salpeter value. NIR and Halpha excess support the existence of a young (< 2
Myr) stellar population of Herbig Ae/Be stars (> 3.0 M_sun) indicating a second
episode of star formation in the cluster region. Using XMM-Newton observations,
we found several X-ray sources in the cluster region but none of the Herbig
Ae/Be stars is detected in X-rays. We compare the distribution of upper limits
for Herbig Ae/Be stars with the X-ray distribution functions of the T-Tauri and
the Herbig Ae/Be stars from previous studies, and found that the X-ray emission
level of these Herbig Ae/Be stars is not more than L_X ~5.2 x 10^{30} erg/s,
which is not significantly higher than for the T-Tauri stars. Therefore, X-ray
emission from Herbig Ae/Be stars could be the result of either unresolved
companion stars or a process similar to T-Tauri stars. We report an extended
X-ray emission from the cluster region NGC 7419, with a total L_X estimate of ~
1.8 x 10^31 erg/s/arcmin^2. Investigation of dust and CO map of 1 degree region
around the cluster indicates the presence of a foreground dust cloud which is
most likely associated with star forming region Sh2-154. This cloud harbors
uniformly distributed pre main sequence stars (0.1-2.0M_sun) and the star
formation in this cloud depend mostly upon the primordial fragmentation.
