Context. Pulsars and their environments represent a major class of Galactic γ-ray sources. Their complex evolution, shaped by the interactions of the pulsar outflow with both the supernova remnant (SNR) and the surrounding interstellar medium (ISM), produces diverse morphological and spectral characteristics observable from radio to PeV energies. Aims. This work aims to collect and homogenise data from all major operating TeV observatories, presenting the first comprehensive catalogue of TeV γ-ray properties of pulsar environments, and facilitating systematic studies of the evolution of pulsar wind nebulae and pulsar halos. Methods. The catalogue was created from information regarding all γ-ray sources that have been classified as pulsar-associated sources in published results from H.E.S.S., MAGIC, VERITAS, HAWC, and LHAASO. For each source, the observed γ-ray properties were cross-matched with pulsar properties from the ATNF catalogue and Fermi-LAT pulsar catalogue. This information was then used to predict the surface brightness for powerful pulsars around which no nebula has been detected yet. Results. The final catalogue comprises all currently known TeV sources associated with pulsars, as seen by different instruments, spanning all evolutionary stages. The sample consists of 128 γ-ray sources, connected to 66 different pulsars. It reflects that the TeV-detected population is dominated by young and energetic pulsars located near the Galactic plane, but includes a growing number of middle-aged systems detected as extended halos. Only a weak correlation is found between TeV luminosity and pulsar characteristic age, indicating that TeV evolution is driven by environmental and transport effects rather than by spin-down age alone. Additionally, five pulsars that should host a PWN detectable by CTAO are identified as prime targets for future observation to improve our under-standing of properties inhibiting the formation of a TeV nebula. Conclusions. This publicly available catalogue provides a uniform foundation for future population studies and for constraining models of particle transport and energy losses in pulsar environments.