We report on H₂ O masers associated with the massive-star forming region G192.16$-$3.84 observed with the new Japanese VLBI network at three epochs spanned for two months, which have revealed the three-dimensional kinematical structure of the whole H₂ O maser region in G192.16$-$3.84, containing two young stellar objects separated by ~ 1200 \,AU. The maser spatio-kinematical structure has well persisted since previous observations, in which the masers are expected to be associated with a highly collimated bipolar jet and an infalling-rotating disk in the northern and southern clusters of H₂ O maser features, respectively. We estimated a jet expansion speed of ~ 100 \,km \,s⁻¹ and re-estimated the dynamical age of the whole jet to be 5.6 × 10⁴ \,yr. We investigated the spatial distribution of the Doppler velocities during the previous and present observations and the relative proper motions of H₂ O maser features in the southern cluster, as well as the relative bulk motion between the two maser clusters. They are well explained by a model of an infalling-rotating disk with a radius of ~ 1000 \,AU and a central stellar mass of 5–10M_, rather than by a model of a bipolar jet perpendicular to the observed CO outflow. Based on the derived H₂ O maser spatio-kinematical parameters, we discuss the formation mechanism of the massive young stellar objects and the outflow development in G192.16$-$3.84.
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