  Coronal jets are ubiquitous in active regions (ARs) and coronal holes. In
this paper, we study a coronal jet related to a C3.4 circular-ribbon flare in
active region 12434 on 2015 October 16. Two minifilaments were located under a
3D fan-spine structure before flare. The flare was generated by the eruption of
one filament. The kinetic evolution of the jet was divided into two phases: a
slow rise phase at a speed of $\sim$131 km s$^{-1}$ and a fast rise phase at a
speed of $\sim$363 km s$^{-1}$ in the plane-of-sky. The slow rise phase may
correspond to the impulsive reconnection at the breakout current sheet. The
fast rise phase may correspond to magnetic reconnection at the flare current
sheet. The transition between the two phases occurred at $\sim$09:00:40 UT. The
blueshifted Doppler velocities of the jet in the Si {\sc iv} 1402.80 {\AA} line
range from -34 to -120 km s$^{-1}$. The accelerated high-energy electrons are
composed of three groups. Those propagating upward along open field generate
type \textrm{III} radio bursts, while those propagating downward produce HXR
emissions and drive chromospheric condensation observed in the Si {\sc iv}
line. The electrons trapped in the rising filament generate a microwave burst
lasting for $\le$40 s. Bidirectional outflows at the base of jet are manifested
by significant line broadenings of the Si {\sc iv} line. The blueshifted
Doppler velocities of outflows range from -13 to -101 km s$^{-1}$. The
redshifted Doppler velocities of outflows range from $\sim$17 to $\sim$170 km
s$^{-1}$. Our multiwavelength observations of the flare-related jet are in
favor of the breakout jet model and are important for understanding the
acceleration and transport of nonthermal electrons.
