  In recent years, observers have found that the fraction of M-stars
demonstrating significant magnetic activity transitions sharply from roughly
$10\%$ for main-sequence stars earlier (more massive) than spectral type M3.5
(0.35 M$_\odot$) to nearly $90\%$ for stars later than M3.5. The latter are
typically rotating quite rapidly, suggesting differing spin-down histories.
Tantalizingly, it is also later than M3.5 at which main-sequence stars become
fully convective, and may no longer contain a tachocline, a layer of rotational
shear revealed by helioseismology to separate the radiative zone (RZ) and
convection zone (CZ). We turn here to the more massive M-stars to study the
impact such a layer may have on their internal dynamics. Using the spherical 3D
MHD simulation code Rayleigh, we compare the properties of convective dynamos
generated within quickly rotating (1, 2, and 4 $\Omega_\odot$) M2 (0.4
M$_\odot$) stars, with the computational domain either terminating at the base
of the convection zone or permitting overshoot into the underlying stable
region. We find that a tachocline is not necessary for the organization of
strong toroidal wreaths of magnetism in these stars, though its presence can
increase the coupling of mean field amplitudes to the stellar rotation rate.
Additionally, in stars that undergo periodic cycles, we find that the presence
of a tachocline tends to make the cycles both longer and more regular than they
would have otherwise been. Finally, we find that the tachocline helps to
enhance the surface poloidal fields and organize them into larger spatial
scales, both of which provide favorable conditions for more rapid angular
momentum loss through a magnetized stellar wind.
