  We present a comprehensive multiwavelength investigation of a likely massive
young cluster `IRAS 05100+3723' and its environment with the aim to understand
its formation history and feedback effects. We find that IRAS 05100+3723 is a
distant ($\sim$3.2 kpc), moderate mass ($\sim$500 \msun), young ($\sim$3 Myr)
cluster with its most massive star being an O8.5V-type. From spectral modeling,
we estimate the effective temperature and log $g$ of the star as $\sim$33,000 K
and $\sim$3.8, respectively. Our radio continuum observations reveal that the
star has ionized its environment forming an HII region of size $\sim$2.7 pc,
temperature $\sim$5,700 K, and electron density $\sim$165 cm$^{-3}$. However,
our large-scale dust maps reveal that it has heated the dust up to several
parsecs ($\sim$10 pc) in the range 17$-$28 K and the morphology of warm dust
emission resembles a bipolar HII region. From dust and $^{13}$CO gas analyses,
we find evidences that the formation of the HII region has occurred at the very
end of a long filamentary cloud around 3 Myr ago, likely due to edge collapse
of the filament. We show that the HII region is currently compressing a clump
of mass $\sim$2700 \msun at its western outskirts, at the junction of the HII
region and filament. We observe several 70 $\mu$m point sources of
intermediate-mass and class 0 nature within the clump. We attribute these
sources as the second generation stars of the complex. We propose that the star
formation in the clump is either induced or being facilitated by the
compression of the expanding HII region onto the inflowing filamentary
material.
