  Intermittency and anisotropy are two important aspects of plasma turbulence,
which the solar wind provides a natural laboratory to investigate. However,
their forms and nature are still under debate, making it difficult to achieve a
consensus in the theoretical interpretation. Here, we perform higher-order
statistics for the observations in the fast solar wind at 1.48 au obtained by
Ulysses and in the slow solar wind at 0.17 au obtained by Parker Solar Probe
(PSP). We find that two subranges clearly exist in the inertial range and they
present distinct features with regard to the intermittency and anisotropy. The
subrange 1 with smaller scale has a multifractal scaling with the second index
$\xi(2) \sim 2/3$ and the subrange 2 with larger scale is also multifractal but
with $\xi(2) \sim 1/2$. The break between two subranges locates at the same
spatial scale for both Ulysses and PSP observations. Subrange 1 is multifractal
in the direction perpendicular to the local magnetic field with $\xi_{\perp}(2)
\sim 2/3$ and seems to be monoscaling in the parallel direction with
$\xi_{\parallel}(2) \sim 1$. Subrange 2 is multifractal in both parallel and
perpendicular directions with $\xi_{\perp}(2) \sim 1/2$ and $\xi_{\parallel}(2)
\sim 2/3$. Both subrange 1 and subrange 2 present power and wavevector
anisotropies. The distinct features of two subranges suggest that a transition
from weak to strong turbulence may occur and the spatial scale of the break may
not evolve with the solar wind expansion. These new results update our
knowledge of the inertial range and provide strong observational constraints on
the understanding of intermittency and anisotropy in solar wind turbulence.
