We study the luminous blue variable candidate J004229.87+410551.8 in the Andromeda galaxy. Previously, the star displayed a spectral anomaly: although the hot emission spectrum was detected, it had strong absorption H and K CaII lines. Subsequently, the object was proposed to be a hot hypergiant or B[e]-supergiant. For the purpose of clear star classification, we conducted spectroscopic and photometric analysis of the object and its surrounding with the help 6-m telescope of SAO RAS, the 3.5-m ARC telescope of the Apache Point Observatory and 2.5-m telescope of the Caucasus Mountain Observatory of Sternberg Astronomical Institute. The spectrum of the object has Balmer emission lines, FeII, [FeII] and [OI] lines. Its spectral energy distribution shows excess in the near-infrared range due to hot circumstellar dust. The indicated features and the high value of estimated star's luminosity ($\log (L/L_{\odot}) = 4.6\pm 0.2$) allow us to finally classify the object as a B[e]-supergiant.