  We present X-ray analysis of the ejecta of supernova remnant G350.1$-$0.3
observed with Chandra and Suzaku, and clarify the ejecta's kinematics over a
decade and obtain a new observational clue to understanding the origin of the
asymmetric explosion. Two images of Chandra X-ray Observatory taken in 2009 and
2018 are analyzed in several methods, and enable us to measure the velocities
in the plane of the sky. A maximum velocity is 4640$\pm$290 km s$^{-1}$
(0.218$\pm$0.014 arcsec yr$^{-1}$) in the eastern region in the remnant. These
findings trigger us to scrutinize the Doppler effects in the spectra of the
thermal emission, and the velocities in the line-of-sight direction are
estimated to be a thousand km s$^{-1}$. The results are confirmed by analyzing
the spectra of Suzaku. Combining the proper motions and line-of-sight
velocities, the ejecta's three-dimensional velocities are $\sim$3000-5000 km
s$^{-1}$. The center of the explosion is more stringently constrained by
finding the optimal time to reproduce the observed spatial expansion. Our
findings that the age of the SNR is estimated at most to be 655 years, and the
CCO is observed as a point source object against the SNR strengthen the
'hydrodynamical kick' hypothesis on the origin of the remnant.
