On the Oosterhoff dichotomy in the Galactic bulge: II. kinematical
  distribution
  We present a kinematical study of RR~Lyrae stars associated with two
Oosterhoff groups in the Galactic bulge. We used data published in the first
paper of the series, plus proper motions from the {\it Gaia} Data Release 2,
and radial velocities from the literature. A 6D kinematical and spatial
solution was obtained for 429 RR~Lyrae stars. We use a model of the Galactic
gravitational potential to infer stellar orbits. We did not find a difference
between the Oosterhoff groups in the individual components of the space
velocity. We report that \textit{foreground} and \textit{background} stars with
respect to the Galactic bulge stand out in the mean $V$ velocity component,
which we interpret as a sign of the Galactic rotation. The movement of the
studied stars in the central region of the Galactic bulge is consistent with
random motions expected for a classical bulge component. From the orbital
integration, we estimate that 8\,\% of the RR~Lyrae stars are halo interlopers
currently located in the Galactic bulge. The majority of the stars' orbits are
within a 3\,kpc radius from the Galactic bulge. The fraction of Oosterhoff\,II
stars increases with increasing Galactic latitude, as well as towards longer
orbital periods. We found several RR~Lyrae stars with high space velocities,
one of which has an extremely long orbital period of $\sim$1\,Gyr. We conclude
that based on their kinematics, the vast majority of the stars in our sample do
not seem to contribute to the boxy/peanut component of the Galactic bulge.
