  Recently, the rapid multiwavelength photometry and flash spectra of supernova
(SN) 2013fs imply that the progenitor stars of regular type II SNe (SNe II)
might be commonly surrounded with a confined dense stellar wind ejected by
themselves with large mass loss rate few years before the SNe. Based on the
assumption that the pre-SN progenitor stars of SNe II have a SN 2013fs-like
wind, with mass loss rate $\dot{M}\sim3\times10^{-3}(v_w/100\rm
km\,s^{-1})M_\odot\rm yr^{-1}$, we investigate the neutrino emission during the
wind breakouts of SN shocks. We find that the regular SNe II can convert a
fraction $\sim10^{-3}$ of their bulk kinetic energy into neutrino emission,
which can contribute a significant fraction of the IceCube-detected neutrino
flux at $\ga300$ TeV. Moreover, the $\la200$~TeV IceCube neutrinos can be
accounted for by cosmic rays produced by the shocks of all SN remnants, losing
energy in their host galaxies, i.e., starburst galaxies. The future follow-up
observations of neutrinos by Gen2 and gamma-rays by CTA and LHAASO from nearby
individual SNe II, within weeks after the explosions, will test this model.
