  We make use of the Parker Solar Probe (PSP) data to explore the nature of
solar wind turbulence focusing on the Alfv\'enic character and power spectra of
the fluctuations and their dependence on distance and context (i.e. large scale
solar wind properties), aiming to understand the role that different effects
such as source properties, solar wind expansion, stream interaction might play
in determining the turbulent state. We carry out a statistical survey of the
data from the first five orbits of PSP with a focus on how the fluctuation
properties at the large, MHD scales, vary with different solar wind streams and
distance from the Sun. A more in-depth analysis from several selected periods
is also presented. Our results show that as fluctuations are transported
outward by the solar wind, the magnetic field spectrum steepens while the shape
of the velocity spectrum remains unchanged. The steepening process is
controlled by the "age" of the turbulence, determined by the wind speed
together with the radial distance. Statistically, faster solar wind has higher
"Alfv\'enicity", with more dominant outward propagating wave component and more
balanced magnetic/kinetic energies. The outward wave dominance gradually
weakens with radial distance, while the excess of magnetic energy is found to
be stronger as we move closer toward the Sun. We show that the turbulence
properties can vary significantly stream to stream even if these streams are of
similar speed, indicating very different origins of these streams. Especially,
the slow wind that originates near the polar coronal holes has much lower
Alfv\'enicity compared with the slow wind that originates from the active
regions/pseudostreamers. We show that structures such as heliospheric current
sheets and velocity shears can play an important role in modifying the
properties of the turbulence.
