  The Solar Orbiter (SO) mission provides the opportunity to study the
evolution of solar wind turbulence. We use SO observations of nine extended
intervals of homogeneous turbulence to determine when turbulent magnetic field
fluctuations may be characterized as: (i) wave-packets and (ii) coherent
structures (CS). We perform the first systematic scale-by-scale decomposition
of the magnetic field using two wavelets known to resolve wave-packets and
discontinuities, the Daubechies 10 (Db10) and Haar respectively. The
probability distributions (pdfs) of turbulent fluctuations on small scales
exhibit stretched tails, becoming Gaussian at the outer scale of the cascade.
Using quantile-quantile plots, we directly compare the wavelet fluctuations
pdfs, revealing three distinct regimes of behaviour. Deep within the inertial
range (IR) both decompositions give essentially the same fluctuation pdfs. Deep
within the kinetic range (KR) the pdfs are distinct as the Haar wavelet
fluctuations have larger variance and more extended tails. On intermediate
scales, spanning the IR-KR break, the pdf is composed of two populations: a
core of common functional form containing $\sim97\%$ of fluctuations, and tails
which are more extended for Haar fluctuations than Db10 fluctuations. This
establishes a crossover between wave-packet (core) and CS (tail) phenomenology
in the IR and KR respectively. The range of scales where the pdfs are
$2$-component is narrow at $0.9$ au ($4-16$ s) and broader ($0.5-8$ s) at $0.4$
au. As CS and wave-wave interactions are both candidates to mediate the
turbulent cascade, these results offer new insights into the distinct physics
of the IR and KR.
