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 (LCs) exhibit the adiabatic cooling envelope emission following the shock breakout up to∼ 14 days from the explosion. SN 2018hna has a rise time of∼ 88 days in the V band, similar to SN 1987A. A 56 Ni mass of∼ 0.087±0.004 M⊙ is inferred for SN 2018hna from its bolometric LC. Hydrodynamical modeling of the cooling phase suggests a progenitor with a radius∼ 50 R⊙, a mass of∼ 14–20 M⊙, and an explosion energy of∼ 1.7–2.9× 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 subsolar metallicity (∼ 0.3 Z⊙) is inferred for the host galaxy UGC 07534, concurrent with the low-metallicity environments of 1987A-like events.