  High cadence ultraviolet, optical and near-infrared photometric and
low-resolution spectroscopic observations of the peculiar Type II supernova
(SN) 2018hna are presented. The early phase multiband light curves exhibit the
adiabatic cooling envelope emission following the shock breakout up to ~14 days
from the explosion. SN~2018hna has a rise time of $\sim$\,88 days in the
V-band, similar to SN 1987A. A $\rm^{56}Ni$ mass of ~0.087$\pm$0.004 $\rm
M_{\odot}$ is inferred for SN 2018hna from its bolometric light curve.
Hydrodynamical modelling of the cooling phase suggests a progenitor with a
radius ~50 $\rm R_{\odot}$, a mass of ~14-20 $\rm M_{\odot}$ and explosion
energy of ~1.7-2.9$\rm \times$ $\rm 10^{51}\ erg$. The smaller inferred radius
of the progenitor than a standard red supergiant is indicative of a blue
supergiant progenitor of SN 2018hna. A sub-solar metallicity (~0.3 $\rm
Z_{\odot}$) is inferred for the host galaxy UGC 07534, concurrent with the
low-metallicity environments of 1987A-like events.
