We analyze high-resolution (Δv ≤ 10 km s−1) optical and infrared spectra covering the O i λ6300 and Ne ii 12.81 m lines from a sample of 31 disks in different evolutionary stages. Following work at optical wavelengths, we use Gaussian profiles to fit the Ne ii lines and classify them into high-velocity component (HVC) or low-velocity component (LVC) if the line centroid is more or less blueshifted than 30 km s−1 with respect to the stellar radial velocity, respectively. Unlike for the O i, where an HVC is often accompanied by an LVC, all 17 sources with an Ne ii detection have either an HVC or an LVC. Ne ii HVCs are preferentially detected toward high accretors ( M yr−1), while LVCs are found in sources with low , low O i luminosity, and large infrared spectral index (n13-31). Interestingly, the Ne ii and O i LVC luminosities display an opposite behavior with n13-31: as the inner dust disk depletes (higher n13-31), the Ne ii luminosity increases while the O i weakens. The Ne ii and O i HVC profiles are generally similar, with centroids and FWHMs showing the expected behavior from shocked gas in microjets. In contrast, the Ne ii LVC profiles are typically more blueshifted and narrower than the O i profiles. The FWHM and centroid versus disk inclination suggest that the Ne ii LVC predominantly traces unbound gas from a slow, wide-angle wind that has not lost completely the Keplerian signature from its launching region. We sketch an evolutionary scenario that could explain the combined O i and Ne ii results and includes screening of hard (∼1 keV) X-rays in inner, mostly molecular, MHD winds.