  The kinematics of the $\epsilon$ Cha young stellar association close to the
Sun has been studied based on a list of candidate stars from the
Dickson-Vandervelde work. The working sample consists of 26 stars with
parallaxes, proper motions from the Gaia~DR3 catalog and radial velocities
taken from literary sources. The orbits of the stars back to the past were
constructed, and the moment when the association had a minimum spatial size was
determined, as well as an analysis of the dependencies of the velocities
$U,V,W$ on the coordinates $x,y,z$ was carried out. It is shown that the
initial sample is divided into two parts with different kinematic properties.
The first sample included 9 stars. Based on the construction of the orbits of
these 9 stars, an age estimate of $t=4.9\pm0.8$ million years was obtained. An
expansion coefficient in the $xz$ plane with the value $K_{xz}=135\pm19$
km/s/kpc was also found for them, on the basis of which another age estimate
$t=7.2\pm1.0$ million years was obtained. The second sample included 17 stars.
The construction of their orbits gave an estimate of age $t=0.2\pm0.3$ million
years, and based on the gradient $\partial W/\partial z=707\pm248$ km/s/kpc, a
second estimate of their age $t=1.4\pm0.5$ million years was obtained. This
suggests that the $\epsilon$ Cha association either consists of two groupings
of different ages, or a younger one arose as a result of a recent outbreak of
star formation within a common star system. The question of the gravitational
connection of the groupings has not been considered in the framework of this
work.
