  Global and semi-global convective dynamo simulations of solar-like stars are
known to show a transition from an anti-solar (fast poles, slow equator) to
solar-like (fast equator, slow poles) differential rotation (DR) for increasing
rotation rate. The dynamo solutions in the latter regime can exhibit regular
cyclic modes, whereas in the former one, only stationary or temporally
irregular solutions have been obtained so far. In this paper we present a
semi-global dynamo simulation in the transition region, exhibiting two
coexisting dynamo modes, a cyclic and a stationary one, both being dynamically
significant. We seek to understand how such a dynamo is driven by analyzing the
large-scale flow properties (DR and meridional circulation) together with the
turbulent transport coefficients obtained with the test-field method. Neither
an $\alpha\Omega$ dynamo wave nor an advection-dominated dynamo are able to
explain the cycle period and the propagation direction of the mean magnetic
field. Furthermore, we find that the $\alpha$ effect is comparable or even
larger than the $\Omega$ effect in generating the toroidal magnetic field, and
therefore, the dynamo seems to be $\alpha^2\Omega$ or $\alpha^2$ type. We
further find that the effective large-scale flows are significantly altered by
turbulent pumping.
