The well-observed type IIP SN 2024bch with the short plateau is shown to be an outcome of the red supergiant explosion with the presupernova mass of $14-15$ $M_{\odot }$ , the explosion energy of $2\times 10^{51}$ erg, and presupernova radius of 1250 $R_{\odot }$ . The early gamma-ray escape demonstrated by the radioactive tail is due to the large 56Ni extension up to 7400 km s−1. The early-time spectral evolution indicates the presence of the circumstellar dense confined envelope with the mass of $0.003-0.006$ $M_{\odot }$ within $6\times 10^{14}$ cm. The deceleration of the outermost ejecta implies the wind with the mass-loss rate of ≈ 6 $\times 10^{-4}$ $M_{\odot }$ yr−1. The inferred mass-loss rate is by one-two order larger compared to most of type IIP supernovae, but comparable to the wind of type IIL SN 1998S. The asymmetry of the broad H $\alpha $ component on day 144 powered by the circumstellar interaction is the outcome of the Thomson scattering and absorption in the Paschen continuum in the unshocked ejecta.
