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We present a comprehensive multiwavelength investigation of a likely massiveyoung cluster `IRAS 05100+3723' and its environment with the aim to understandits formation history and feedback effects. We find that IRAS 05100+3723 is adistant ($\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 Kand $\sim$3.8, respectively. Our radio continuum observations reveal that thestar 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}$. However,our large-scale dust maps reveal that it has heated the dust up to severalparsecs ($\sim$10 pc) in the range 17$-$28 K and the morphology of warm dustemission 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 veryend of a long filamentary cloud around 3 Myr ago, likely due to edge collapseof the filament. We show that the HII region is currently compressing a clumpof mass $\sim$2700 \msun at its western outskirts, at the junction of the HIIregion and filament. We observe several 70 $\mu$m point sources ofintermediate-mass and class 0 nature within the clump. We attribute thesesources as the second generation stars of the complex. We propose that the starformation in the clump is either induced or being facilitated by thecompression of the expanding HII region onto the inflowing filamentarymaterial.

A Comprehensive Study of the Young Cluster IRAS 05100+3723: Properties, Surrounding Interstellar Matter, and Associated Star Formation