  Understanding the characteristics of young stellar populations is essential
for deriving insights into star formation processes within parent molecular
clouds and the influence of massive stars. This study focuses on YSOs in the G
045.49+00.04 molecular cloud, including three UC HII regions. Using infrared
photometric data and radiation models, we identified 1482 YSOs with masses
ranging from 1.5 to 22 Msol. Among these, 315 form dense clusters near IRAS
sources, with high-mass stars responsible for ionization. The non-cluster YSOs
(1168) are uniformly distributed on the field. The distribution of YSOs from
both samples on the colour-magnitude diagram and by the evolutionary ages is
different. About 75% of objects in the IRAS clusters are concentrated around
the ZAMS and have a well-defined peak at an age of Log(Age[years]) = 6.75, with
a narrow spread. The non-cluster objects have two concentrations located to the
right and left of the 0.1 Myr isochrone and two well-defined peaks at Log(Age)
= 6.25 and 5.25. The K luminosity functions alpha slopes for the IRAS clusters
and non-cluster objects are 0.32 and 0.72, respectively. The steeper alpha
slope is suggesting that the non-cluster objects are less evolved, which is
well consistent with the evolutionary age. Similar patterns were observed in
the neighboring G 45.14+00.14 region. The both regions (G 045.49+00.04 and G
45.14+00.14) are located and distinguished by their brightness and density at
the edge of the bubble around the highly variable X-ray binary GRS 1915+105,
which includes a black hole and a K-giant companion. Based on the above, we can
assume that the process of star formation in the young IRAS clusters was
triggered by the GRS 915+105-initiated shock front inside the ISM massive
condensation, through the process of "collecting and collapse". Most
non-cluster objects probably belong to a later generation.
