  To probe the star formation (SF) process, we present a thorough
multi-wavelength investigation of several H II regions located toward l = 24.8
deg, b = 0.1 deg. A system of at least five H II regions including the
mid-infrared bubble N36 (hereafter "system N36"; extension ~35 pc) is
observationally investigated, and is located at a distance of 6.0 kpc. With
this distance, the system N36 is found to be situated at the interface of the
Galactic bar and the Norma Galactic arm in our Galaxy, where one may expect the
collisions of molecular clouds due to the bar potential. Each H II region
(dynamical age ~0.4 - 1.3 Myr) in the system is powered by an O-type star. The
system contains 27 ATLASGAL dust clumps at 870 micron. Several clumps are
massive (> 10^3 M_sun), and have high bolometric luminosity (> 10^3 L_sun).
Using the GRS 13CO line data, in the direction of the system N36, two velocity
components are found around 109 and 113 km/s, and are linked in the velocity
space. The morphological analysis of 13CO favours the presence of interacting
molecular clouds in the system. Four H II regions and two 6.7 GHz masers are
spatially observed at the common areas of the two clouds. The analysis of the
Spitzer photometric data also traces the noticeable SF activity in the system.
Considering the observational outcomes, the formation of O-type stars
(including ongoing SF) in the system appears to be triggered by the collisions
of molecular clouds at the bar-arm interface.
