  We have observed the three low-mass protostars, IRAS 15398$-$3359, L1527 IRS
and TMC-1A, with the ALMA 12-m array, the ACA 7-m array, and the IRAM-30m and
APEX telescopes in the C$^{18}$O $J=2$-1 emission. Overall, the C$^{18}$O
emission shows clear velocity gradients at radii of $\sim$100-1000 au, which
likely originate from rotation of envelopes, while velocity gradients are less
clear and velocity structures are more perturbed on scales of $\sim$1000-10,000
au. IRAS 15398$-$3359 and L1527 IRS show a break at radii of $\sim$1200 and
$\sim$1700 au in the radial profile of the peak velocity, respectively. The
peak velocity is proportional to $r^{-1.38}$ or $r^{-1.7}$ within the break
radius, which can be interpreted as indicating a rotational motion of the
envelope with a degree of contamination of gas motions on larger spatial
scales. The peak velocity follows $v_\mathrm{peak} \propto r^{0.68}$ or
$v_\mathrm{peak} \propto r^{0.46}$ outside the break radius, which is similar
to the $J/M$-$R$ relation of dense cores. TMC-1A exhibits the radial profile of
the peak velocity not consistent with the rotational motion of the envelope nor
the $J/M$-$R$ relation. The origin of the relation of $v_\mathrm{peak} \propto
r^{0.46\operatorname{-}0.68}$ is investigated by examining correlations of the
velocity deviation ($\delta v$) and the spatial scale ($\tau$) in the two
sources. Obtained spatial correlations, $\delta v \propto \tau^{\sim0.6}$, are
consistent with the scaling law predicted by turbulence models, which may
suggest the large-scale velocity structures originate from turbulence.
