We report the results of astrometric VLBI observations toward the Mira variable star BX�Cam using the VERA VLBI array. The observation was performed from 2012 February to 2014 November. The parallax obtained is 1.73 � 0.03 mas corresponding to a distance of 0.58 � 0.01 kpc. The parallax of this source was reported in Gaia DR2 as 4.13 � 0.25 mas, and there is a 240% difference between these two measurements. Astrometric results from our VLBI observations show that we exactly traced the angular motions of the seven maser spots in BX�Cam. We calculated the stellar luminosities using both parallaxes, and obtained luminosities of and . These deduced luminosities also support the validity of the parallax that we determined with VERA. Evaluating the two parallaxes, we conclude that the parallax of 1.73 � 0.03 mas from the VERA observations is correct for BX�Cam. We obtained the systemic motion of BX�Cam as (μ_αcos δ^sys, ) = (13.48 � 0.14, −34.30 � 0.18) mas yr⁻¹. The total of 73 H₂O maser spots detected from our VLBI observations shows a spatial distribution of 30 au � 80 au, with a strong elongation along the north–south direction. They show outflows with a three-dimensional velocity of 14.79 � 1.40 km s⁻¹. From a comparison between the time variations of the V-band magnitudes and the H₂O masers, we found that the variation of the H₂O masers is relevant to that seen in the V band even though the H₂O masers do not recover their maximum flux in each cycle.